Equatorial periodic orbits and gravitational waveforms in a black hole free of Cauchy horizon

TL;DR

This study investigates periodic orbits and gravitational waveforms in a black hole system lacking a Cauchy horizon, revealing how external parameters influence orbital dynamics and waveform phases, with implications for black hole parameter constraints.

Contribution

It introduces analysis of periodic orbits and gravitational waveforms in a novel black hole spacetime without Cauchy horizons, highlighting deviations from Schwarzschild cases and potential observational signatures.

Findings

Orbital radius, angular momentum, and energy increase with the hair parameter.

Gravitational waveforms capture zoom-whirl behavior and phase shifts.

Waveform phase advances compared to Schwarzschild black holes.

Abstract

In this paper, we study the periodic orbits and gravitational wave radiation in an extreme mass ratio inspiral system, where a stellar-mass object orbits a supermassive black hole without Cauchy horizons. Firstly, by using the effective potential, the marginally bound orbits and the innermost stable circular orbits are investigated. It is found that the radius, orbital angular momentum, and energy increase with the hair parameter for both orbits. Based on these results, we examine one special type of orbit, the periodic orbit, around the black hole without the Cauchy horizon. The results show that, for a fixed rational number, the energy and angular momentum of the periodic orbit increase with the hair parameter. In particular, we observe a significant deviation from the Schwarzschild case for small hair parameter with a large amount of external mass outside the black hole horizon. Moreover, we examine the waveforms in the extreme mass ratio inspiral system to explore the orbital information of the periodic orbits and the constraints on the parameters of the black holes. The results reveal that the gravitational waveforms can fully capture the zoom-whirl behavior of periodic orbits. Moreover, the phase of the gravitational waves imposes constraints on the parameters of the black hole solutions. As the system evolves, the phase shift of the waveforms becomes increasingly significant, with cumulative deviations becoming more pronounced over time. Compared to the Schwarzschild black hole background, the waveform phase will advance for the central supermassive black hole without a Cauchy horizon.